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HINODE Operation Plan (HOP)

accepted on

27-feb-2025

 HOP No.

  HOP title

HOP 0497
[SOOP: burst SOOP] Solar Orbiter & DKIST coordinated observation

plan term

2025/04/01-2025/04/01

 　 　

proposer

  name : Barczynski, Janitzek 　  e-mail : krzysztof.barczynski[at]pmodwrc.ch, nils.janitzek[at]pmodwrc.ch

contact person in HINODE team

  name : Kobelski, Duncan (NASA/MSFC) / Watanabe (NAOJ) / De Pontieu (LMSAL), SOT -- DeRosa/Dick Shine (LMSAL), SOT -- Okamoto (NAOJ), XRT -- Reeves/Paola Testa (SAO), XRT -- Shimojo (NAOJ), EIS -- Matthews/Len Culhane (UCL/MSSL), EIS -- Warren/Ignacio Ugarte-Urra (NRL), EIS -- Watanabe (NAOJ) 　  e-mail : adam.kobelski[at]nasa.gov, jessie.m.duncan[at]nasa.gov, tet_watanabe[at]jcom.zaq.ne.jp, bdp[at]lmsal.com, derosa[at]lmsal.com, shine[at]lmsal.com, joten.okamoto[at]nao.ac.jp, kreeves[at]cfa.harvard.edu, ptesta[at]cfa.harvard.edu, masumi.shimojo[at]nao.ac.jp, sarah.matthews[at]ucl.ac.uk, harry.warren[at]nrl.navy.mil, j.culhane[at]ucl.ac.uk, ignacio.ugarteurra[at]nrl.navy.mil

 abstract of observational proposal
Main Objective: Upflow region at AR border

Scientific Justification: The upflow regions at the boundaries of active regions may be potential sources of the slow solar wind. However, the mechanisms driving plasma flow in these coronal upflow regions and the underlying layers of the solar atmosphere remain open questions. This study aims to understand the mechanisms responsible for plasma upflow at the borders of coronal active regions. To achieve this, we propose coordinated observations involving Solar Orbiter, DKIST, IRIS, and Hinode.

 request to SOT
Fast Map, Full FOV 1 side CCD Q75; FOV 314"x162" at 19:00 UT on 1st April 2025.

 request to XRT
XRT would run a 30s cadence two filter (Al_poly, Be_thin) program for the short primary window (19-19:40). For the remainder of the time (18:00 -22:00 UT), cadence can be reduced as needed to fit telemetry.

 request to EIS
We would like observation mode: study ID number 133 (CAM_ARTB_RHESSI_a_1); at least core spectral lines; continuous raster; the observation mode should be repeated continously at least between 19:00 and 19:40 UT on 1st April 2025; if telemetry allows the observation should be repeated between 18:00 and 22:00 on 1st April 2025.

 other participating instruments
IRIS requests:
We will submit proposal to the IRIS team.

Additional instrument coordination:
SOLAR ORBITER, SOOP:R_SMALL_HRES_HCAD_RS-burst, https://s2e2.cosmos.esa.int/confluence/display/SOSP/R_SMALL_HRES_HCAD_RS-burst;

DKIST

 remarks
Dates: The most important is to provide a coordinated observation between DKIST, Solar Orbiter (high-resolution instrument) and IRIS: start time: 1 April 2025 19:00 UT - end time: 1st April 2025 19:40 UT. It is possible to extend the coordinated observation time to provide a coordination between DKIST, IRIS and Hinode: start time: 1st April 2025 18:00 UT and end time: 1st April 2024 22:00 UT.

Time window:
Minimum duration time window: 1st April 2025 19:00 UT - end time: 1st April 2025 19:40 UT containting coordinated observation with DKIST, Solar Orbiter (high-resolution instruments) and IRIS;
Extended time windows: 1st April 2025 18:00 UT - end time: 1st April 2025 22:00 UT containing coordinated observation with DKIST and IRIS. Short interruptions during minimum duration time window are not recommended, but during extended time window are allowed.

Target(s) of interest: Upflow region at an active region borders, close to disk centre

Previous HOPs:
HOP0492- sucessfull coordination of AR and upflow region observation using IRIS, Hinode and Solar Orbiter. The highest temporal cadence observation of Solar Orbiter EUI/HRI with cadence of 1 sec. DKIST didn't observed due to poor weather condition.

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